AN 08-10-209 BC-348 series Radio Receiver (maintenance)

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Bridle, A. H. 1967. Monthly Notices Roy. Astron. 136:219. - - . 1968. Doctoral thesis. Cambridge University. Burbidge, G. R. 1970. Ann. Rev. Astron. 8:369. Burke, B. 1967. lAU Symposium No. 31, p. 361. Daniel, R. , and S. A. Stephens. 1970. Space Sei. Rev. 10:599. , and A. Maxwell. 1966. Astrophys. J. 146:653. - - , and A. H. M. Martin. 1971. Nature 223: 112. Elliott, K. H. 1970. Nature 226: 1236. Ginzburg, V. , and S. I. Syrovatsky. 1964. The Origin 0/ Cosmic Rays. New York: Macmillan. 1965. Ann.

Burton (1972) has suggested that within our Galaxy the data can be interpreted as if the HI is optically thin. 15) 29 but the Doppler' broadening produced by thermal motions in the clouds gives the line a finite width. Other motions within the clouds, such as turbulence, rotation, expansion, and contraction, will also produce line broadening. In Chapter 4 the effects of streaming as a broadening mechanism are discussed. Within each cloud the atoms have a Maxwellian velocity distribution due to their thermal motions, which means that the numbers at.

And H. H. Aumann. 1970. Astrophys. 162:179. Mathewson, D. S. 1968. J. 163:147. - - - , and D. K. Milne, 1965. AustralianJ. Phys. 18:635. Merkelijn, J. , and M. M. Davis. 1967. Eull. Astron. Inst. Neth. 19:246. Mills, B. Y. 1959. Proc. U. Symposium. No. 9, New York: Academic Press, p. 431. PachoIczyk, A. G. 1970. Radio Astrophysics. San Francisco: W. H. Freeman. Pawsey, J. L. 1961. In Galactic Structure, A. Blaauw and M. Schmidt, eds. Chicago: University of Chicago Press, p. 219. Piddington, J.

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